The new nebula in LDN 1415 – A cry from the cradle of a low-luminosity source

Stecklum, B.; Melnikov, S.; Meusinger, H.

doi:10.1051/0004-6361:20065433

Cited by 16 publications

(28 citation statements)

References 34 publications

(39 reference statements)

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“…The spectrum of HH 892A resembles to that of a high excitation HHO (Raga & Canto, 1996). An active Herbig-Haro flow towards L1415 has also been reported by Stecklum et al (2007) based on the longslit spectroscopic study. On the DSS image of L1415, a HHO candidate near IRAS 04376+5413 was detected (Stecklum et al, 2007).…”

Section: L1415supporting

confidence: 58%

“…An active Herbig-Haro flow towards L1415 has also been reported by Stecklum et al (2007) based on the longslit spectroscopic study. On the DSS image of L1415, a HHO candidate near IRAS 04376+5413 was detected (Stecklum et al, 2007). Using subsequent Hα and [SII] imaging, Stecklum et al (2007) confirmed the presence of the emission line object with no counterpart.…”

Section: L1415mentioning

confidence: 53%

“…The embedded L1415-IRS is found to be associated with HHOs (Stecklum et al, 2007). HHOs (Herbig, 1950;Haro, 1952) are the tracers of pre-main-sequence stars (Reipurth & Bally, 2001).…”

Section: Outflow Direction and Magnetic Fieldsmentioning

confidence: 91%

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Probing the magnetic fields in L1415 and L1389

Soam

Lee

Maheswar

et al. 2016

Mon. Not. R. Astron. Soc.

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We present the R-band polarimetric results towards two nebulae L1415 and L1389 containing low luminosity stars. Aim of this study is to understand the role played by magnetic fields in formation of low luminosity objects. Linear polarization arise due to dichroism of the background starlight projected on the cloud providing the plane-of-the sky magnetic field orientation. The offsets between mean magnetic field directions obtained towards L1415 and L1389 and the projected outflow axes are found to be 35• and 12• , respectively. The offset between cloud minor axes and mean envelope magnetic field direction in L1415 and L1389 are 50• and 87• , respectively. To estimate the magnetic field strength by using the updated Chandrasekhar-Fermi relation, we obtained the 12 CO(J=1-0) line velocity dispersion value towards L1415 cloud using the TRAO single dish observations. The values of B pos in L1415 and L1389 are found to be 28 µG and 149 µG using CF technique and 23 µG and 140 µG using structure function analysis, respectively. The values of B pos in these clouds are found to be consistent using both the techniques. By combining the present results with those obtained from our previous study of magnetic fields in cores with VeLLOs, we attempt to improve the sample of cores with low luminosity protostars and bridge the gap between the understanding of importance of magnetic fields in cores with VeLLOs and low luminosity protostars. The Results of this work and that of our previous work show that the outflow directions are aligned with envelope magnetic fields of the clouds.

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Section: L1415supporting

confidence: 58%

Section: L1415mentioning

confidence: 53%

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Probing the magnetic fields in L1415 and L1389

Soam

Lee

Maheswar

et al. 2016

Mon. Not. R. Astron. Soc.

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“…In contrast to the previous results, a Chandra observation was unable to detect the outburst source that illuminates the new nebula associated with IRAS 04376+5413 in LDN 1415, located at d ∼ 170 pc (Kastner et al 2006a;Stecklum 2006;Stecklum et al 2007).…”

Section: Introductionmentioning

confidence: 59%

A few days before the end of the 2008 extreme outburst of EX Lupi: accretion shocks and a smothered stellar corona unveiled by XMM-Newton

Grosso

Hamaguchi

Kastner

et al. 2010

A&A

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Context. EX Lup is a pre-main sequence star that exhibits repetitive and irregular optical outbursts driven by an increase in the mass accretion rate in its circumstellar disk. In mid-January 2008, EX Lup, the prototype of the small class of eruptive variables called EXors, began an extreme outburst that lasted seven months. Aims. We attempt to characterize the X-ray and UV emission of EX Lup during this outburst. Methods. We observed EX Lup during about 21 h with XMM-Newton, simultaneously in X-rays and UV, on August 10-11, 2008 -a few days before the end of its 2008 outburst -when the optical flux of EX Lup remained about 4 times above its pre-outburst level. Results. We detected EX Lup in X-rays with an observed flux in the 0.2-10 keV energy range of 5.4 × 10 −14 erg s −1 cm −2 during a low-level period. This observed flux increased by a factor of four during a flaring period that lasted about 2 h. The observed spectrum of the low-level period is dominated below ∼1.5 keV by emission from a relatively cool plasma (∼4.7 MK) that is lightly absorbed (N H 3.6 × 10 20 cm −2 ) and above ∼1.5 keV by emission from a plasma that is ∼ten times hotter and affected by a photoelectric absorption that is 75 times larger. The intrinsic X-ray luminosity of the relatively cool plasma is ∼4 × 10 28 erg s −1 . The intrinsic X-ray luminosity of EX Lup, ∼3.4 × 10 29 erg s −1 , is hence dominated by emission from the hot plasma. During the X-ray flare, the emission measure and the intrinsic X-ray luminosity of this absorbed plasma component is five times higher than during the low-level period. We detected UV variability on timescales ranging from less than one hour up to about four hours. We show from simulated light curves that the power spectral density of the UV light curve can be modeled with a red-noise spectrum with a power-law index of 1.39 ± 0.06. None of the UV events observed on August 10-11, 2008 correlate unambiguously with simultaneous X-ray peaks. Conclusions. The soft X-ray spectral component is most likely associated with accretion shocks, as opposed to jet activity, given the absence of forbidden emission lines of low-excitation species (e.g., [O i]) in optical spectra of EX Lup obtained during outburst. The hard X-ray spectral component, meanwhile, is most likely associated with a smothered stellar corona. The UV emission is reminiscent of accretion events, such as those already observed with the Optical/UV Monitor from other accreting pre-main sequence stars, and is evidently dominated by emission from accretion hot spots. The large photoelectric absorption of the active stellar corona is most likely due to high-density gas above the corona in accretion funnel flows.

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“…Thus we conclude that this object, Fig. 4 SED of the candidate proto-brown dwarf (Stecklum et al 2007). The line displays the SED of L1014-IRS (Young et al 2004) for comparison BHR111-IR, is likely driving the outflow.…”

Section: Bhr111-a Starless Core Remains Starless?mentioning

confidence: 79%

Herbig-Haro objects—tracers of the formation of low-mass stars and sub-stellar objects

Stecklum

Meusinger

Froebrich

2007

Astrophys Space Sci

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Herbig-Haro objects (HHOs) are caused by outflows from young objects. Since the outflow relies on mass accretion from a circumstellar disk, it indicates ongoing growth. Recent results of infrared observations yielded evidence for disks around brown dwarfs. This suggests that at least a certain fraction of brown dwarfs forms like stars. Thus, young sub-stellar objects might cause HHOs as well. We present selected results of a general survey for HHOs based on DSS-II plates and CCD images taken with the Tautenburg Schmidt telescope. Numerous young objects could be identified due to their association with newly detected HHOs. In some cases the luminosity is consistent with very low-mass stars or close to sub-stellar values. This holds for L1415-IRS and a few infrared sources embedded in other dark clouds (e.g., GF9, BHR111). The question on the minimum mass for outflow activity is addressed.

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The new nebula in LDN 1415 – A cry from the cradle of a low-luminosity source

Cited by 16 publications

References 34 publications

Probing the magnetic fields in L1415 and L1389

Probing the magnetic fields in L1415 and L1389

A few days before the end of the 2008 extreme outburst of EX Lupi: accretion shocks and a smothered stellar corona unveiled by XMM-Newton

Herbig-Haro objects—tracers of the formation of low-mass stars and sub-stellar objects

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